The Subaru Deep Field: The Optical Imaging Data

Kashikawa, Nobunari; Shimasaku, Kazuhiro; Yasuda, Naoki; Ajiki, Masaru; Akiyama, Masayuki; Ando, Hiroyasu; Aoki, Kentaro; Doi, Mamoru; Fujita, Shinobu S.; Furusawa, Hisanori; Hayashino, T.; Iwamuro, Fumihide; Iye, Masanori; Karoji, Hiroshi; Kobayashi, Naoto; Kodaira, Keiichi; Kodama, Tadayuki; Komiyama, Yutaka; Matsuda, Yoshihisa; Miyazaki, Satoshi; Mizumoto, Y.; Morokuma, Tomoki; Motohara, Kentaro; Murayama, Takashi; Nagao, Tohru; Nariai, Kyoji; Ohta, Kouji; Okamura, S.; Ouchi, Masami; Sasaki, Toshiyuki; Sato, Yasunori; Sekiguchi, K.; Shioya, Y.; Tamura, H.; Taniguchi, Yoshiaki; Umemura, Masayuki; Yamada, Tōru; Yoshida, Makiko

doi:10.1093/pasj/56.6.1011

Cited by 150 publications

(113 citation statements)

References 34 publications

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“…The Subaru deep survey projects, including SXDS (Furusawa et al 2008) and the Subaru Deep Field (SDF; Kashikawa et al 2004), have been very successful in searching for z 6  galaxies. SXDS consists of five Suprime-Cam pointings (Figure 1), and covers ∼1.2 deg 2 in total (Furusawa et al 2008).…”

Section: The Sxds Fieldmentioning

confidence: 99%

A Magellan M2FS Spectroscopic Survey of Galaxies at 5.5 < z < 6.8: Program Overview and a Sample of the Brightest Lyα Emitters

Jiang

Shen

Bian

et al. 2017

ApJ

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We present a spectroscopic survey of high-redshift, luminous galaxies over four square degrees on the sky, aiming to build a large and homogeneous sample of Lyα emitters (LAEs) at z 5.7 » and 6.5, and Lyman-break galaxies (LBGs) at z 5.5 6.8 < <. The fields that we choose to observe are well studied, such as by the Subaru XMMNewton Deep Survey and COSMOS. They have deep optical imaging data in a series of broad and narrow bands, allowing for the efficient selection of galaxy candidates. Spectroscopic observations are being carried out using the multi-object spectrograph M2FS on the Magellan Clay telescope. M2FS is efficient enough to identify highredshift galaxies, owing to its 256 optical fibers deployed over a circular field of view 30¢ in diameter. We have observed ∼2.5 square degrees. When the program is completed, we expect to identify more than 400 bright LAEs at z 5.7 » and 6.5, and a substantial number of LBGs at z 6  . This unique sample will be used to study a variety of galaxy properties and to search for large protoclusters. Furthermore, the statistical properties of these galaxies will be used to probe cosmic reionization. We describe the motivation, program design, target selection, and M2FS observations. We also outline our science goals, and present a sample of the brightest LAEs at z 5.7 » and 6.5. This sample contains 32 LAEs with Lyα luminosities higher than 10 43 erg s −1 . A few of them reach 3×10 43 erg s −1 , comparable to the two most luminous LAEs known at z 6  , "CR7" and "COLA1." These LAEs provide ideal targets to study extreme galaxies in the distant universe.

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Section: The Sxds Fieldmentioning

confidence: 99%

A Magellan M2FS Spectroscopic Survey of Galaxies at 5.5 < z < 6.8: Program Overview and a Sample of the Brightest Lyα Emitters

Jiang

Shen

Bian

et al. 2017

ApJ

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“…For the GOODS-N, we used archival raw B-and V-band images (Capak et al 2004). For the SDF and SXDS fields, we used public, reduced B-and V-band images (Kashikawa et al 2004;Furusawa et al 2008).…”

Section: O B S E Rvat I O N S a N D Data R E D U C T I O Nmentioning

confidence: 99%

The Subaru Lyα blob survey: a sample of 100-kpc Lyα blobs at z = 3

Matsuda

Yamada

Hayashino

et al. 2011

Monthly Notices of the Royal Astronomical Society: Letters

133

166

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We present results of a survey for giant Lyα blobs (LABs) at z= 3 with Subaru/Suprime‐Cam. We obtained Lyα imaging at z= 3.09 ± 0.03 around the SSA22 protocluster and in several blank fields. The total survey area is 2.1 deg2, corresponding to a comoving volume of 1.6 × 106 Mpc3. Using a uniform detection threshold of 1.4 × 10−18 erg s−1 cm−2 arcsec−2 for the Lyα images, we construct a sample of 14 LAB candidates with major‐axis diameters larger than 100 kpc, including five previously known blobs and two known quasars. This survey triples the number of known LABs over 100 kpc. The giant LAB sample shows a possible ‘morphology–density relation’: filamentary LABs reside in average density environments as derived from compact Lyα emitters, while circular LABs reside in both average density and overdense environments. Although it is hard to examine the formation mechanisms of LABs only from the Lyα morphologies, more filamentary LABs may relate to cold gas accretion from the surrounding intergalactic medium (IGM) and more circular LABs may relate to large‐scale gas outflows, which are driven by intense starbursts and/or by active galactic nucleus activities. Our survey highlights the potential usefulness of giant LABs to investigate the interactions between galaxies and the surrounding IGM from the field to overdense environments at high redshift.

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“…GALAXYCOUNT uses a default sigmoid with a = 3.0 which may be used to provide an estimate of the expected completeness of any observation by scaling b appropriately. The b values were measured from the SDF B−, R-and I-completeness functions in Kashikawa et al (2004), and converted to Vega magnitudes using the transformations given in Section 2.4 (U was derived from the B band completeness function), and the SDF K-band completeness function was measured from Maihara et al (2001). In order to allow scaling from the SDF observations, we have taken throughputs for Suprime-Cam BRI (actually i ) from Miyazaki et al (2002) (convolved with Mauna Kea atmospheric transmission from Hook et al 2004), and for CISCO K from Motohara et al (2002), we have assumed the Gemini Multi-object Spectrograph (GMOS) throughput for U.…”

Section: Completenessmentioning

confidence: 99%

GalaxyCount: a java calculator of galaxy counts and variances in multiband wide-field surveys to 28 AB mag

Ellis

Bland-Hawthorn

2007

Monthly Notices of the Royal Astronomical Society

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We provide a consistent framework for estimating galaxy counts and variances in wide‐field images for a range of photometric bands. The variances include both Poissonian noise and variations due to large‐scale structure. We demonstrate that our statistical theory is consistent with the counts in the deepest multiband surveys available. The statistical estimates depend on several observational parameters (e.g. seeing, signal‐to‐noise ratio), and include a sophisticated treatment of detection completeness. The java calculator is freely available1 and offers the user the option to adopt our consistent framework or a different scheme. We also provide a summary table of statistical measures in the different bands for a range of different fields of view. Reliable estimation of the background counts has profound consequences in many areas of observational astronomy. We provide two such examples. One is from a recent study of the Sculptor galaxy NGC 300 where stellar photometry has been used to demonstrate that the outer disc extends to 10 effective radii, far beyond what was thought possible for a normal low‐luminosity spiral. We confirm this finding by a re‐analysis of the background counts. Secondly, we determine the luminosity function of the galaxy cluster Abell 2734, both through spectroscopically determined cluster membership, and through statistical subtraction of the background galaxies using the calculator and offset fields. We demonstrate very good agreement, suggesting that expensive spectroscopic follow‐up, or off‐source observations, may often be bypassed via determination of the galaxy background with GalaxyCount.

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The Subaru Deep Field: The Optical Imaging Data

Cited by 150 publications

References 34 publications

A Magellan M2FS Spectroscopic Survey of Galaxies at 5.5 < z < 6.8: Program Overview and a Sample of the Brightest Lyα Emitters

A Magellan M2FS Spectroscopic Survey of Galaxies at 5.5 < z < 6.8: Program Overview and a Sample of the Brightest Lyα Emitters

The Subaru Lyα blob survey: a sample of 100-kpc Lyα blobs at z = 3

GalaxyCount: a java calculator of galaxy counts and variances in multiband wide-field surveys to 28 AB mag

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